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Motoba T, Sitnov MI, Stephens GK, Gershman DJ. A New Perspective on Magnetotail Electron and Ion Divergent Flows: MMS Observations. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2022; 127:e2022JA030514. [PMID: 36591322 PMCID: PMC9788156 DOI: 10.1029/2022ja030514] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/01/2022] [Revised: 08/17/2022] [Accepted: 09/13/2022] [Indexed: 06/17/2023]
Abstract
Fast divergent flows of electrons and ions in the magnetotail plasma sheet are conventionally interpreted as a key reconnection signature caused by the magnetic topology change at the X-line. Therefore, reversals of the x-component (V x⊥) of the plasma flow perpendicular to the magnetic field must correlate with the sign changes in the north-south component of the magnetic field (B z ). Here we present observations of the flow reversals that take place with no correlated B z reversals. We report six such events, which were measured with the high-resolution plasma and fields instruments of the Magnetospheric Multiscale mission. We found that electron flow reversals in the absence of B z reversals (a) have amplitudes of ∼1,000-2,000 km s-1 and durations of a few seconds; (b) are embedded into larger-scale ion flow reversals with enhanced ion agyrotropy; and (c) compared with conventional reconnection outflows around the electron diffusion regions (EDRs), have less (if ever) pronounced electron agyrotropy, dawnward electron flow amplitude, and electric field strength toward the neutral sheet, although their energy conversion parameters, including the Joule heating rate, are quite substantial. These results suggest that such flow reversals develop in the ion-demagnetization regions away from electron-scale current sheets, in particular the EDRs, and yet they play an important role in the energy conversion. These divergent flows are interpreted as precursors of the flow-driven reconnection onsets provided by the ion tearing or the ballooning/interchange instability.
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Affiliation(s)
- T. Motoba
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - M. I. Sitnov
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - G. K. Stephens
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
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Turbulent current sheet frozen in bursty bulk flow: observation and model. Sci Rep 2022; 12:15547. [PMID: 36109607 PMCID: PMC9478094 DOI: 10.1038/s41598-022-19266-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/02/2022] [Accepted: 08/26/2022] [Indexed: 11/16/2022] Open
Abstract
Utilizing four-point joint observations by Magnetospheric Multiscale Spacecraft (MMS), we investigate the main features of the current sheet frozen in (CSFI) the bursty bulk flow. Typical event on the steady long-lasting BBF on July 23, 2017 shows the enhanced dawn-dusk current (Jy0) in the CSFI (β ~ 10). The magnitude of the Jy0 in the CSFI is about 5.5 nA/m2. The CSFI is highly turbulent, with the ratio of ∆J/J0 of ~ 2 (where ∆J is perturbed J). The turbulent CSFI is characterized by intermittent current coherent structures. The magnitude of the spiky-J at coherent structures is typically above 30 nA/m2. Spectrum analysis exhibits that BBF turbulence follows distinct dissipation laws inside and outside the CSFI. Based on MMS observations, we propose a new model of the BBF in the framework of magnetohydrodynamics. In this model, the BBF is depicted as a closed plasma system with the localized current sheet frozen at the center of the flow (Taylor’s hypothesis). In the light of principle of Helmholtz-decomposition, the BBF motion in the tail plasma sheet is explained. The model also predicts the thermal expansion of the BBF after leaving the reconnection source region.
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3
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Baker DN. Wave-particle interaction effects in the Van Allen belts. EARTH, PLANETS, AND SPACE : EPS 2021; 73:189. [PMID: 34720651 PMCID: PMC8550337 DOI: 10.1186/s40623-021-01508-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/04/2021] [Accepted: 08/24/2021] [Indexed: 06/13/2023]
Abstract
Discovering such structures as the third radiation belt (or "storage ring") has been a major observational achievement of the NASA Radiation Belt Storm Probes program (renamed the "Van Allen Probes" mission in November 2012). A goal of that program was to understand more thoroughly how high-energy electrons are accelerated deep inside the radiation belts-and ultimately lost-due to various wave-particle interactions. Van Allen Probes studies have demonstrated that electrons ranging up to 10 megaelectron volts (MeV) or more can be produced over broad regions of the outer Van Allen zone on timescales as short as a few minutes. The key to such rapid acceleration is the interaction of "seed" populations of ~ 10-200 keV electrons (and subsequently higher energies) with electromagnetic waves in the lower band (whistler-mode) chorus frequency range. Van Allen Probes data show that "source" electrons (in a typical energy range of one to a few tens of keV energy) produced by magnetospheric substorms play a crucial role in feeding free energy into the chorus waves in the outer zone. These chorus waves then, in turn, rapidly heat and accelerate the tens to hundreds of keV seed electrons injected by substorms to much higher energies. Hence, we often see that geomagnetic activity driven by strong solar storms (coronal mass ejections, or CMEs) commonly leads to ultra-relativistic electron production through the intermediary step of waves produced during intense magnetospheric substorms. More generally, wave-particle interactions are of fundamental importance over a broad range of energies and in virtually all regions of the magnetosphere. We provide a summary of many of the wave modes and particle interactions that have been studied in recent times.
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Affiliation(s)
- Daniel N. Baker
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, 3665 Discovery Drive, 600 UCB, Boulder, CO 80303 USA
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Ghaffari R, Cully CM, Gabrielse C. Statistical Study of Whistler-Mode Waves and Expected Pitch Angle Diffusion Rates During Dispersionless Electron Injections. GEOPHYSICAL RESEARCH LETTERS 2021; 48:e2021GL094085. [PMID: 35864943 PMCID: PMC9286036 DOI: 10.1029/2021gl094085] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/28/2021] [Revised: 08/05/2021] [Accepted: 08/10/2021] [Indexed: 06/15/2023]
Abstract
Energetic electron injections can generate or amplify electromagnetic waves such as whistler-mode waves. These waves can resonantly interact with available particles to affect their equatorial pitch angle. This process can be considered as a diffusion that scatters particles into the loss cone. This study investigates whistler-mode wave generation in conjunction with electron injections using in situ wave measurements by the Time History of Events and Macroscale Interactions during Substorms mission during 2011-2020. We characterize the whistler-mode wave behavior associated with 733 selected dispersionless electron injections and dipolarizing flux bundles (DFBs). We observe intense wave activity and strong diffusion associated with only the top 5% and 10% of the selected injection events, respectively. We also study the wave activity when there is a sharp rise in the northward component of the magnetic field around the injection time (DFBs). In this case, the generated wave powers increase, and the power change is at least two times greater than non-DFB injections.
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Affiliation(s)
- R. Ghaffari
- Department of Physics and AstronomyUniversity of CalgaryCalgaryALCanada
| | - C. M. Cully
- Department of Physics and AstronomyUniversity of CalgaryCalgaryALCanada
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Sitnov M, Birn J, Ferdousi B, Gordeev E, Khotyaintsev Y, Merkin V, Motoba T, Otto A, Panov E, Pritchett P, Pucci F, Raeder J, Runov A, Sergeev V, Velli M, Zhou X. Explosive Magnetotail Activity. SPACE SCIENCE REVIEWS 2019; 215:31. [PMID: 31178609 PMCID: PMC6528807 DOI: 10.1007/s11214-019-0599-5] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/05/2018] [Accepted: 04/27/2019] [Indexed: 06/01/2023]
Abstract
Modes and manifestations of the explosive activity in the Earth's magnetotail, as well as its onset mechanisms and key pre-onset conditions are reviewed. Two mechanisms for the generation of the pre-onset current sheet are discussed, namely magnetic flux addition to the tail lobes, or other high-latitude perturbations, and magnetic flux evacuation from the near-Earth tail associated with dayside reconnection. Reconnection onset may require stretching and thinning of the sheet down to electron scales. It may also start in thicker sheets in regions with a tailward gradient of the equatorial magnetic field B z ; in this case it begins as an ideal-MHD instability followed by the generation of bursty bulk flows and dipolarization fronts. Indeed, remote sensing and global MHD modeling show the formation of tail regions with increased B z , prone to magnetic reconnection, ballooning/interchange and flapping instabilities. While interchange instability may also develop in such thicker sheets, it may grow more slowly compared to tearing and cause secondary reconnection locally in the dawn-dusk direction. Post-onset transients include bursty flows and dipolarization fronts, micro-instabilities of lower-hybrid-drift and whistler waves, as well as damped global flux tube oscillations in the near-Earth region. They convert the stretched tail magnetic field energy into bulk plasma acceleration and collisionless heating, excitation of a broad spectrum of plasma waves, and collisional dissipation in the ionosphere. Collisionless heating involves ion reflection from fronts, Fermi, betatron as well as other, non-adiabatic, mechanisms. Ionospheric manifestations of some of these magnetotail phenomena are discussed. Explosive plasma phenomena observed in the laboratory, the solar corona and solar wind are also discussed.
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Affiliation(s)
- Mikhail Sitnov
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | | | | | - Evgeny Gordeev
- Earth’s Physics Department, Saint Petersburg State University, St. Petersburg, Russia
| | | | - Viacheslav Merkin
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - Tetsuo Motoba
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | | | - Evgeny Panov
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Philip Pritchett
- Department of Physics and Astronomy, University of California, Los Angeles, CA USA
| | - Fulvia Pucci
- National Institute for Fusion Science, National Institutes of Natural Sciences, Toki, 509-5292 Japan
- Princeton Plasma Physics Laboratory, Princeton University, Princeton, NJ USA
| | - Joachim Raeder
- Institute for the Study of Earth, Oceans and Space, University of New Hampshire, Durham, NH USA
| | - Andrei Runov
- Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA USA
| | - Victor Sergeev
- Earth’s Physics Department, Saint Petersburg State University, St. Petersburg, Russia
| | - Marco Velli
- University of California Los Angeles, Los Angeles, CA 90095 USA
| | - Xuzhi Zhou
- School of Earth and Space Sciences, Peking University, Beijing, 100871 China
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Sandhu JK, Rae IJ, Freeman MP, Forsyth C, Gkioulidou M, Reeves GD, Spence HE, Jackman CM, Lam MM. Energization of the Ring Current by Substorms. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2018; 123:8131-8148. [PMID: 30775195 PMCID: PMC6360953 DOI: 10.1029/2018ja025766] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/11/2018] [Revised: 08/10/2018] [Accepted: 09/12/2018] [Indexed: 06/01/2023]
Abstract
The substorm process releases large amounts of energy into the magnetospheric system, although where the energy is transferred to and how it is partitioned remains an open question. In this study, we address whether the substorm process contributes a significant amount of energy to the ring current. The ring current is a highly variable region, and understanding the energization processes provides valuable insight into how substorm-ring current coupling may contribute to the generation of storm conditions and provide a source of energy for wave driving. In order to quantify the energy input into the ring current during the substorm process, we analyze Radiation Belt Storm Probes Ion Composition Experiment and Helium Oxygen Proton Electron ion flux measurements for H+, O+, and He+. The energy content of the ring current is estimated and binned spatially for L and magnetic local time. The results are combined with an independently derived substorm event list to perform a statistical analysis of variations in the ring current energy content with substorm phase. We show that the ring current energy is significantly higher in the expansion phase compared to the growth phase, with the energy enhancement persisting into the substorm recovery phase. The characteristics of the energy enhancement suggest the injection of energized ions from the tail plasma sheet following substorm onset. The local time variations indicate a loss of energetic H+ ions in the afternoon sector, likely due to wave-particle interactions. Overall, we find that the average energy input into the ring current is ∼9% of the previously reported energy released during substorms.
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Affiliation(s)
- J K Sandhu
- Department of Space and Climate Physics, Mullard Space Science Laboratory University College London London UK
| | - I J Rae
- Department of Space and Climate Physics, Mullard Space Science Laboratory University College London London UK
| | | | - C Forsyth
- Department of Space and Climate Physics, Mullard Space Science Laboratory University College London London UK
| | - M Gkioulidou
- Applied Physics Laboratory Johns Hopkins University Baltimore MD USA
| | - G D Reeves
- Los Alamos National Laboratory Los Alamos NM USA
| | - H E Spence
- Institute for the Study of Earth, Oceans, and Space University of New Hampshire Durham NH USA
| | - C M Jackman
- Department of Physics and Astronomy University of Southampton Southampton UK
| | - M M Lam
- Department of Physics and Astronomy University of Southampton Southampton UK
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Murphy KR, Inglis AR, Sibeck DG, Rae IJ, Watt CEJ, Silveira M, Plaschke F, Claudepierre SG, Nakamura R. Determining the Mode, Frequency, and Azimuthal Wave Number of ULF Waves During a HSS and Moderate Geomagnetic Storm. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2018; 123:6457-6477. [PMID: 31681521 PMCID: PMC6813628 DOI: 10.1029/2017ja024877] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/11/2017] [Revised: 05/15/2018] [Accepted: 05/17/2018] [Indexed: 06/10/2023]
Abstract
Ultralow frequency (ULF) waves play a fundamental role in the dynamics of the inner magnetosphere and outer radiation belt during geomagnetic storms. Broadband ULF wave power can transport energetic electrons via radial diffusion, and discrete ULF wave power can energize electrons through a resonant interaction. Using observations from the Magnetospheric Multiscale mission, we characterize the evolution of ULF waves during a high-speed solar wind stream (HSS) and moderate geomagnetic storm while there is an enhancement of the outer radiation belt. The Automated Flare Inference of Oscillations code is used to distinguish discrete ULF wave power from broadband wave power during the HSS. During periods of discrete wave power and utilizing the close separation of the Magnetospheric Multiscale spacecraft, we estimate the toroidal mode ULF azimuthal wave number throughout the geomagnetic storm. We concentrate on the toroidal mode as the HSS compresses the dayside magnetosphere resulting in an asymmetric magnetic field topology where toroidal mode waves can interact with energetic electrons. Analysis of the mode structure and wave numbers demonstrates that the generation of the observed ULF waves is a combination of externally driven waves, via the Kelvin-Helmholtz instability, and internally driven waves, via unstable ion distributions. Further analysis of the periods and toroidal azimuthal wave numbers suggests that these waves can couple with the core electron radiation belt population via the drift resonance during the storm. The azimuthal wave number and structure of ULF wave power (broadband or discrete) have important implications for the inner magnetospheric and radiation belt dynamics.
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Affiliation(s)
- Kyle R. Murphy
- Department of AstronomyUniversity of MarylandCollege ParkMDUSA
| | | | - David G. Sibeck
- NASA Goddard Space Flight Center, Space Weather Laboratory (674)GreenbeltMDUSA
| | - I. Jonathan Rae
- Department of Space and Climate Physics, Mullard Space Science LaboratoryUniversity College LondonLondonUK
| | | | | | | | | | - Rumi Nakamura
- Space Research InstituteAustrian Academy of SciencesGrazAustria
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8
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Nikoukar R, Lawrence DJ, Peplowski PN, Dewey RM, Korth H, Baker DN, McNutt RL. Statistical Study of Mercury's Energetic Electron Events as Observed by the Gamma-Ray and Neutron Spectrometer Instrument Onboard MESSENGER. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2018; 123:4961-4978. [PMID: 30167351 PMCID: PMC6108406 DOI: 10.1029/2018ja025339] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/09/2018] [Revised: 04/17/2018] [Accepted: 05/11/2018] [Indexed: 06/08/2023]
Abstract
We present results from a statistical analysis of Mercury's energetic electron (EE) events as observed by the gamma-ray and neutron spectrometer instrument onboard the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. The main objective of this study is to investigate possible anisotropic behavior of EE events using multiple data sets from MESSENGER instruments. We study the data from the neutron spectrometer (NS) and the gamma-ray spectrometer anticoincidence shield (ACS) because they use the same type of borated plastic scintillator and, hence, they have very similar response functions, and their large surface areas make them more sensitive to low-intensity EE events than MESSENGER's particle instrumentation. The combined analysis of NS and ACS data reveals two different classes of energetic electrons: "Standard" events and "ACS-enhanced" events. Standard events, which comprise over 90% of all events, have signal sizes that are the same in both the ACS and NS. They are likely gyrating particles about Mercury's magnetic field following a 90° pitch angle distribution and are located in well-defined latitude and altitude regions within Mercury's magnetosphere. ACS-enhanced events, which comprise less than 10% of all events, have signal sizes in the ACS that are 10 to 100 times larger than those observed by the NS. They follow a beam-like distribution and are observed both inside and outside Mercury's magnetosphere with a wider range of latitudes and altitudes than Standard events. The difference between the Standard and ACS-enhanced event characteristics suggests distinct underyling acceleration mechanisms.
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Affiliation(s)
- Romina Nikoukar
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | | | | | - Ryan M. Dewey
- Department of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMIUSA
| | - Haje Korth
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - Daniel N. Baker
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | - Ralph L. McNutt
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
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Kiehas SA, Runov A, Angelopolos V, Hietala H, Korovinksiy D. Magnetotail Fast Flow Occurrence Rate and Dawn-Dusk Asymmetry at X GSM ∼ -60 R E. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2018; 123:1767-1778. [PMID: 29780679 PMCID: PMC5947117 DOI: 10.1002/2017ja024776] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/12/2017] [Revised: 12/28/2017] [Accepted: 01/11/2018] [Indexed: 06/02/2023]
Abstract
As a direct result of magnetic reconnection, plasma sheet fast flows act as primary transporter of mass, flux, and energy in the Earth's magnetotail. During the last decades, these flows were mainly studied within XGSM>-60RE , as observations near or beyond lunar orbit were limited. By using 5 years (2011-2015) of ARTEMIS (Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moons Interaction with the Sun) data, we statistically investigate earthward and tailward flows at around 60 RE downtail. A significant fraction of fast flows is directed earthward, comprising 43% (vx >400 km/s) to 56% (vx >100 km/s) of all observed flows. This suggests that near-Earth and midtail reconnection are equally probable of occurring on either side of the ARTEMIS downtail distance. For fast convective flows (v⊥x >400 km/s), this fraction of earthward flows is reduced to about 29%, which is in line with reconnection as source of these flows and a downtail decreasing Alfvén velocity. More than 60% of tailward convective flows occur in the dusk sector (as opposed to the dawn sector), while earthward convective flows are nearly symmetrically distributed between the two sectors for low AL (>-400 nT) and asymmetrically distributed toward the dusk sector for high AL (<-400 nT). This indicates that the dawn-dusk asymmetry is more pronounced closer to Earth and moves farther downtail during high geomagnetic activity. This is consistent with similar observations pointing to the asymmetric nature of tail reconnection as the origin of the dawn-dusk asymmetry of flows and other related observables. We infer that near-Earth reconnection is preferentially located at dusk, whereas midtail reconnection (X >- 60RE ) is likely symmetric across the tail during weak substorms and asymmetric toward the dusk sector for strong substorms, as the dawn-dusk asymmetric nature of reconnection onset in the near-Earth region progresses downtail.
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Affiliation(s)
- S. A. Kiehas
- Space Research InstituteAustrian Academy of SciencesGrazAustria
| | - A. Runov
- Institute of Geophysics and Planetary Physics, Department of Earth, Planetary, and Space SciencesUniversity of CaliforniaLos AngelesCAUSA
| | - V. Angelopolos
- Institute of Geophysics and Planetary Physics, Department of Earth, Planetary, and Space SciencesUniversity of CaliforniaLos AngelesCAUSA
| | - H. Hietala
- Institute of Geophysics and Planetary Physics, Department of Earth, Planetary, and Space SciencesUniversity of CaliforniaLos AngelesCAUSA
| | - D. Korovinksiy
- Space Research InstituteAustrian Academy of SciencesGrazAustria
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10
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Kilpua E, Koskinen HEJ, Pulkkinen TI. Coronal mass ejections and their sheath regions in interplanetary space. LIVING REVIEWS IN SOLAR PHYSICS 2017; 14:5. [PMID: 31997985 PMCID: PMC6956910 DOI: 10.1007/s41116-017-0009-6] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/02/2017] [Accepted: 10/03/2017] [Indexed: 06/09/2023]
Abstract
Interplanetary coronal mass ejections (ICMEs) are large-scale heliospheric transients that originate from the Sun. When an ICME is sufficiently faster than the preceding solar wind, a shock wave develops ahead of the ICME. The turbulent region between the shock and the ICME is called the sheath region. ICMEs and their sheaths and shocks are all interesting structures from the fundamental plasma physics viewpoint. They are also key drivers of space weather disturbances in the heliosphere and planetary environments. ICME-driven shock waves can accelerate charged particles to high energies. Sheaths and ICMEs drive practically all intense geospace storms at the Earth, and they can also affect dramatically the planetary radiation environments and atmospheres. This review focuses on the current understanding of observational signatures and properties of ICMEs and the associated sheath regions based on five decades of studies. In addition, we discuss modelling of ICMEs and many fundamental outstanding questions on their origin, evolution and effects, largely due to the limitations of single spacecraft observations of these macro-scale structures. We also present current understanding of space weather consequences of these large-scale solar wind structures, including effects at the other Solar System planets and exoplanets. We specially emphasize the different origin, properties and consequences of the sheaths and ICMEs.
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Affiliation(s)
- Emilia Kilpua
- Department of Physics, University of Helsinki, Helsinki, Finland
| | - Hannu E. J. Koskinen
- Department of Physics, University of Helsinki, Helsinki, Finland
- Finnish Meteorological Institute, Espoo, Finland
| | - Tuija I. Pulkkinen
- Department of Electronics and Nanoengineering, Aalto University, Espoo, Finland
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Yao Z, Pu ZY, Rae IJ, Radioti A, Kubyshkina MV. Auroral streamer and its role in driving wave-like pre-onset aurora. GEOSCIENCE LETTERS 2017; 4:8. [PMID: 32215237 PMCID: PMC7067272 DOI: 10.1186/s40562-017-0075-6] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/26/2016] [Accepted: 04/04/2017] [Indexed: 06/10/2023]
Abstract
The time scales of reconnection outflow, substorm expansion, and development of instabilities in the terrestrial magnetosphere are comparable, i.e., from several to tens of minutes, and their existence is related. In this paper, we investigate the physical relations among those phenomena with measurements during a substorm event on January 29, 2008. We present conjugate measurements from ground-based high-temporal resolution all-sky imagers and in situ THEMIS measurements. An auroral streamer (north-south aligned thin auroral layer) was formed and propagated equatorward, which usually implies an earthward propagating plasma flow in the magnetotail. At the most equatorward part of the auroral streamer, a wave-like auroral band was formed aligning in the east-west direction. The wave-like auroral structure is usually explained as a consequence of instability development. Using AM03 model, we trace the auroral structure to magnetotail and estimate a wavelength of ~0.5 R E. The scale is comparable to the drift mode wavelength determined by the in situ measurements from THEMIS-A, whose footpoint is on the wave-like auroral arc. We also present similar wave-like aurora observations from Cassini ultraviolet imaging spectrograph at Saturn and from Hubble space telescope at Jupiter, suggesting that the wave-like aurora structure is likely a result of fundamental plasma dynamics in the solar system planetary magnetospheres.
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Affiliation(s)
- Zhonghua Yao
- Laboratoire de Physique Atmosphérique et Planétaire, STAR institute, Université de Liège, Liège, Belgium
- School of Earth and Space Sciences, Peking University, Beijing, China
- UCL Mullard Space Science Laboratory, Dorking, RH5 6NT UK
| | - Z. Y. Pu
- School of Earth and Space Sciences, Peking University, Beijing, China
| | - I. J. Rae
- UCL Mullard Space Science Laboratory, Dorking, RH5 6NT UK
| | - A. Radioti
- Laboratoire de Physique Atmosphérique et Planétaire, STAR institute, Université de Liège, Liège, Belgium
| | - M. V. Kubyshkina
- Physics Faculty, St. Petersburg State University, St. Petersburg, Russia
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Jordanova VK, Tu W, Chen Y, Morley SK, Panaitescu A, Reeves GD, Kletzing CA. RAM-SCB simulations of electron transport and plasma wave scattering during the October 2012 "double-dip" storm. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2016; 121:8712-8727. [PMID: 27867801 PMCID: PMC5101868 DOI: 10.1002/2016ja022470] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/01/2016] [Revised: 08/31/2016] [Accepted: 09/03/2016] [Indexed: 06/06/2023]
Abstract
Mechanisms for electron injection, trapping, and loss in the near-Earth space environment are investigated during the October 2012 "double-dip" storm using our ring current-atmosphere interactions model with self-consistent magnetic field (RAM-SCB). Pitch angle and energy scattering are included for the first time in RAM-SCB using L and magnetic local time (MLT)-dependent event-specific chorus wave models inferred from NOAA Polar-orbiting Operational Environmental Satellites (POES) and Van Allen Probes Electric and Magnetic Field Instrument Suite and Integrated Science observations. The dynamics of the source (approximately tens of keV) and seed (approximately hundreds of keV) populations of the radiation belts simulated with RAM-SCB is compared with Van Allen Probes Magnetic Electron Ion Spectrometer observations in the morning sector and with measurements from NOAA 15 satellite in the predawn and afternoon MLT sectors. We find that although the low-energy (E< 100 keV) electron fluxes are in good agreement with observations, increasing significantly by magnetospheric convection during both SYM-H dips while decreasing during the intermediate recovery phase, the injection of high-energy electrons is underestimated by this mechanism throughout the storm. Local acceleration by chorus waves intensifies the electron fluxes at E≥50 keV considerably, and RAM-SCB simulations overestimate the observed trapped fluxes by more than an order of magnitude; the precipitating fluxes simulated with RAM-SCB are weaker, and their temporal and spatial evolutions agree well with POES/Medium Energy Proton and Electron Detectors data.
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Affiliation(s)
- V. K. Jordanova
- Space Science and ApplicationsLos Alamos National LaboratoryLos AlamosNew MexicoUSA
| | - W. Tu
- Space Science and ApplicationsLos Alamos National LaboratoryLos AlamosNew MexicoUSA
- Department of Physics and AstronomyWest Virginia UniversityMorgantownWest VirginiaUSA
| | - Y. Chen
- Space Science and ApplicationsLos Alamos National LaboratoryLos AlamosNew MexicoUSA
| | - S. K. Morley
- Space Science and ApplicationsLos Alamos National LaboratoryLos AlamosNew MexicoUSA
| | - A.‐D. Panaitescu
- Space Science and ApplicationsLos Alamos National LaboratoryLos AlamosNew MexicoUSA
| | - G. D. Reeves
- Space Science and ApplicationsLos Alamos National LaboratoryLos AlamosNew MexicoUSA
| | - C. A. Kletzing
- Department of Physics and AstronomyUniversity of IowaIowa CityIowaUSA
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13
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Baker DN, Dewey RM, Lawrence DJ, Goldsten JO, Peplowski PN, Korth H, Slavin JA, Krimigis SM, Anderson BJ, Ho GC, McNutt RL, Raines JM, Schriver D, Solomon SC. Intense energetic electron flux enhancements in Mercury's magnetosphere: An integrated view with high-resolution observations from MESSENGER. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2016; 121:2171-2184. [PMID: 27830111 PMCID: PMC5076489 DOI: 10.1002/2015ja021778] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/07/2015] [Revised: 11/20/2015] [Accepted: 12/22/2015] [Indexed: 06/06/2023]
Abstract
The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury has provided a wealth of new data about energetic particle phenomena. With observations from MESSENGER's Energetic Particle Spectrometer, as well as data arising from energetic electrons recorded by the X-Ray Spectrometer and Gamma-Ray and Neutron Spectrometer (GRNS) instruments, recent work greatly extends our record of the acceleration, transport, and loss of energetic electrons at Mercury. The combined data sets include measurements from a few keV up to several hundred keV in electron kinetic energy and have permitted relatively good spatial and temporal resolution for many events. We focus here on the detailed nature of energetic electron bursts measured by the GRNS system, and we place these events in the context of solar wind and magnetospheric forcing at Mercury. Our examination of data at high temporal resolution (10 ms) during the period March 2013 through October 2014 supports strongly the view that energetic electrons are accelerated in the near-tail region of Mercury's magnetosphere and are subsequently "injected" onto closed magnetic field lines on the planetary nightside. The electrons populate the plasma sheet and drift rapidly eastward toward the dawn and prenoon sectors, at times executing multiple complete drifts around the planet to form "quasi-trapped" populations.
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Affiliation(s)
- Daniel N Baker
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Colorado USA
| | - Ryan M Dewey
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Colorado USA
| | - David J Lawrence
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA
| | - John O Goldsten
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA
| | | | - Haje Korth
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA
| | - James A Slavin
- Department of Atmospheric, Oceanic and Space Sciences University of Michigan Ann Arbor Michigan USA
| | - Stamatios M Krimigis
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA; Office of Space Research and Technology Academy of Athens Athens Greece
| | - Brian J Anderson
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA
| | - George C Ho
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA
| | - Ralph L McNutt
- The Johns Hopkins University Applied Physics Laboratory Laurel Maryland USA
| | - Jim M Raines
- Department of Atmospheric, Oceanic and Space Sciences University of Michigan Ann Arbor Michigan USA
| | - David Schriver
- Department of Physics and Astronomy University of California Los Angeles California USA
| | - Sean C Solomon
- Department of Terrestrial Magnetism Carnegie Institution of Washington Washington District of Columbia USA; Lamont-Doherty Earth Observatory Columbia University Palisades New York USA
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14
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Kalmoni NME, Rae IJ, Watt CEJ, Murphy KR, Forsyth C, Owen CJ. Statistical characterization of the growth and spatial scales of the substorm onset arc. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2015; 120:8503-8516. [PMID: 27867792 PMCID: PMC5111420 DOI: 10.1002/2015ja021470] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/18/2015] [Revised: 09/14/2015] [Accepted: 09/19/2015] [Indexed: 06/02/2023]
Abstract
We present the first multievent study of the spatial and temporal structuring of the aurora to provide statistical evidence of the near-Earth plasma instability which causes the substorm onset arc. Using data from ground-based auroral imagers, we study repeatable signatures of along-arc auroral beads, which are thought to represent the ionospheric projection of magnetospheric instability in the near-Earth plasma sheet. We show that the growth and spatial scales of these wave-like fluctuations are similar across multiple events, indicating that each sudden auroral brightening has a common explanation. We find statistically that growth rates for auroral beads peak at low wave number with the most unstable spatial scales mapping to an azimuthal wavelength λ≈ 1700-2500 km in the equatorial magnetosphere at around 9-12 RE . We compare growth rates and spatial scales with a range of theoretical predictions of magnetotail instabilities, including the Cross-Field Current Instability and the Shear Flow Ballooning Instability. We conclude that, although the Cross-Field Current instability can generate similar magnitude of growth rates, the range of unstable wave numbers indicates that the Shear Flow Ballooning Instability is the most likely explanation for our observations.
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Affiliation(s)
- N. M. E. Kalmoni
- Mullard Space Science LaboratoryUniversity College LondonDorkingUK
| | - I. J. Rae
- Mullard Space Science LaboratoryUniversity College LondonDorkingUK
| | - C. E. J. Watt
- Department of MeteorologyUniversity of ReadingReadingUK
| | - K. R. Murphy
- NASA Goddard Space Flight CenterGreenbeltMarylandUSA
| | - C. Forsyth
- Mullard Space Science LaboratoryUniversity College LondonDorkingUK
| | - C. J. Owen
- Mullard Space Science LaboratoryUniversity College LondonDorkingUK
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15
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Dai L, Wang C, Duan S, He Z, Wygant JR, Cattell CA, Tao X, Su Z, Kletzing C, Baker DN, Li X, Malaspina D, Blake JB, Fennell J, Claudepierre S, Turner DL, Reeves GD, Funsten HO, Spence HE, Angelopoulos V, Fruehauff D, Chen L, Thaller S, Breneman A, Tang X. Near-Earth injection of MeV electrons associated with intense dipolarization electric fields: Van Allen Probes observations. GEOPHYSICAL RESEARCH LETTERS 2015; 42:6170-6179. [PMID: 27656009 PMCID: PMC5014237 DOI: 10.1002/2015gl064955] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/15/2015] [Revised: 07/15/2015] [Accepted: 07/16/2015] [Indexed: 05/17/2023]
Abstract
Substorms generally inject tens to hundreds of keV electrons, but intense substorm electric fields have been shown to inject MeV electrons as well. An intriguing question is whether such MeVelectron injections can populate the outer radiation belt. Here we present observations of a substorm injection of MeV electrons into the inner magnetosphere. In the premidnight sector at L ∼ 5.5, Van Allen Probes (Radiation Belt Storm Probes)-A observed a large dipolarization electric field (50 mV/m) over ∼40 s and a dispersionless injection of electrons up to ∼3 MeV. Pitch angle observations indicated betatron acceleration of MeV electrons at the dipolarization front. Corresponding signals of MeV electron injection were observed at LANL-GEO, THEMIS-D, and GOES at geosynchronous altitude. Through a series of dipolarizations, the injections increased the MeV electron phase space density by 1 order of magnitude in less than 3 h in the outer radiation belt (L > 4.8). Our observations provide evidence that deep injections can supply significant MeV electrons.
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Affiliation(s)
- Lei Dai
- State Key Laboratory of Space Weather, National Space Science Center Chinese Academy of Sciences Beijing China; School of Physics and Astronomy University of Minnesota, Twin Cities Minneapolis Minnesota USA
| | - Chi Wang
- State Key Laboratory of Space Weather, National Space Science Center Chinese Academy of Sciences Beijing China
| | - Suping Duan
- State Key Laboratory of Space Weather, National Space Science Center Chinese Academy of Sciences Beijing China
| | - Zhaohai He
- State Key Laboratory of Space Weather, National Space Science Center Chinese Academy of Sciences Beijing China
| | - John R Wygant
- School of Physics and Astronomy University of Minnesota, Twin Cities Minneapolis Minnesota USA
| | - Cynthia A Cattell
- School of Physics and Astronomy University of Minnesota, Twin Cities Minneapolis Minnesota USA
| | - Xin Tao
- Department of Geophysics and Planetary Sciences University of Science and Technology of China Hefei China
| | - Zhenpeng Su
- Department of Geophysics and Planetary Sciences University of Science and Technology of China Hefei China
| | - Craig Kletzing
- Department of Physics and Astronomy University of Iowa Iowa City Iowa USA
| | - Daniel N Baker
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
| | - Xinlin Li
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
| | - David Malaspina
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
| | - J Bernard Blake
- Space Sciences Department The Aerospace Corporation Los Angeles California USA
| | - Joseph Fennell
- Space Sciences Department The Aerospace Corporation Los Angeles California USA
| | - Seth Claudepierre
- Space Sciences Department The Aerospace Corporation Los Angeles California USA
| | - Drew L Turner
- Space Sciences Department The Aerospace Corporation Los Angeles California USA
| | | | | | - Harlan E Spence
- Department of Physics Institute for Earth, Oceans and Space University of New Hampshire Durham New Hampshire USA
| | - Vassilis Angelopoulos
- Department of Earth, Planetary and Space Sciences and Institute of Geophysics and Planetary Physics University of California Los Angeles California USA
| | - Dennis Fruehauff
- Institute of Geophysics and extraterrestrial Physics Braunschweig University of Technology Braunschweig Germany
| | - Lunjin Chen
- Department of Physics University Of Texas at Dallas Richardson Texas USA
| | - Scott Thaller
- School of Physics and Astronomy University of Minnesota, Twin Cities Minneapolis Minnesota USA
| | - Aaron Breneman
- School of Physics and Astronomy University of Minnesota, Twin Cities Minneapolis Minnesota USA
| | - Xiangwei Tang
- School of Physics and Astronomy University of Minnesota, Twin Cities Minneapolis Minnesota USA
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16
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Artemyev AV, Vasiliev AA. Resonant ion acceleration by plasma jets: Effects of jet breaking and the magnetic-field curvature. PHYSICAL REVIEW. E, STATISTICAL, NONLINEAR, AND SOFT MATTER PHYSICS 2015; 91:053104. [PMID: 26066269 DOI: 10.1103/physreve.91.053104] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/20/2014] [Indexed: 06/04/2023]
Abstract
In this paper we consider resonant ion acceleration by a plasma jet originating from the magnetic reconnection region. Such jets propagate in the background magnetic field with significantly curved magnetic-field lines. Decoupling of ion and electron motions at the leading edge of the jet results in generation of strong electrostatic fields. Ions can be trapped by this field and get accelerated along the jet front. This mechanism of resonant acceleration resembles surfing acceleration of charged particles at a shock wave. To describe resonant acceleration of ions, we use adiabatic theory of resonant phenomena. We show that particle motion along the curved field lines significantly influences the acceleration rate. The maximum gain of energy is determined by the particle's escape from the system due to this motion. Applications of the proposed mechanism to charged-particle acceleration in the planetary magnetospheres and the solar corona are discussed.
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Affiliation(s)
- A V Artemyev
- Space Research Institute (IKI) 117997, 84/32 Profsoyuznaya Str, Moscow, Russia
| | - A A Vasiliev
- Space Research Institute (IKI) 117997, 84/32 Profsoyuznaya Str, Moscow, Russia
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17
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Angelopoulos V, Runov A, Zhou XZ, Turner DL, Kiehas SA, Li SS, Shinohara I. Electromagnetic Energy Conversion at Reconnection Fronts. Science 2013; 341:1478-82. [DOI: 10.1126/science.1236992] [Citation(s) in RCA: 204] [Impact Index Per Article: 18.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
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18
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Nagai T, Machida S. Magnetic Reconnection in the Near-Earth Magnetotail. ACTA ACUST UNITED AC 2013. [DOI: 10.1029/gm105p0211] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/18/2023]
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19
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20
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Shay MA, Drake JF, Eastwood JP, Phan TD. Super-Alfvénic propagation of substorm reconnection signatures and Poynting flux. PHYSICAL REVIEW LETTERS 2011; 107:065001. [PMID: 21902330 DOI: 10.1103/physrevlett.107.065001] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/01/2010] [Indexed: 05/31/2023]
Abstract
The propagation of reconnection signatures and their associated energy are examined using kinetic particle-in-cell simulations and Cluster satellite observations. It is found that the quadrupolar out-of-plane magnetic field near the separatrices is associated with a kinetic Alfvén wave. For magnetotail parameters, the parallel propagation of this wave is super-Alfvénic (V(∥) ∼ 1500-5500 km/s) and generates substantial Poynting flux (S ∼ 10(-5)-10(-4) W/m(2)) consistent with Cluster observations of magnetic reconnection. This Poynting flux substantially exceeds that due to frozen-in ion bulk outflows and is sufficient to generate white light aurora in Earth's ionosphere.
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Affiliation(s)
- M A Shay
- Department of Physics and Astronomy, University of Delaware, Newark, 19716, USA.
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21
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A current filamentation mechanism for breaking magnetic field lines during reconnection. Nature 2011; 474:184-7. [PMID: 21633355 DOI: 10.1038/nature10091] [Citation(s) in RCA: 120] [Impact Index Per Article: 9.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/22/2010] [Accepted: 04/01/2011] [Indexed: 11/09/2022]
Abstract
During magnetic reconnection, the field lines must break and reconnect to release the energy that drives solar and stellar flares and other explosive events in space and in the laboratory. Exactly how this happens has been unclear, because dissipation is needed to break magnetic field lines and classical collisions are typically weak. Ion-electron drag arising from turbulence, dubbed 'anomalous resistivity', and thermal momentum transport are two mechanisms that have been widely invoked. Measurements of enhanced turbulence near reconnection sites in space and in the laboratory support the anomalous resistivity idea but there has been no demonstration from measurements that this turbulence produces the necessary enhanced drag. Here we report computer simulations that show that neither of the two previously favoured mechanisms controls how magnetic field lines reconnect in the plasmas of greatest interest, those in which the magnetic field dominates the energy budget. Rather, we find that when the current layers that form during magnetic reconnection become too intense, they disintegrate and spread into a complex web of filaments that causes the rate of reconnection to increase abruptly. This filamentary web can be explored in the laboratory or in space with satellites that can measure the resulting electromagnetic turbulence.
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22
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Morioka A, Miyoshi Y, Tsuchiya F, Misawa H, Kasaba Y, Asozu T, Okano S, Kadokura A, Sato N, Miyaoka H, Yumoto K, Parks GK, Honary F, Trotignon JG, Décréau PME, Reinisch BW. On the simultaneity of substorm onset between two hemispheres. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010ja016174] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- A. Morioka
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - Y. Miyoshi
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - F. Tsuchiya
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - H. Misawa
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - Y. Kasaba
- Geophysical Institute; Tohoku University; Sendai Japan
| | - T. Asozu
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
- Japan Atomic Energy Agency; Ibaraki Japan
| | - S. Okano
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - A. Kadokura
- National Institute of Polar Research; Tokyo Japan
| | - N. Sato
- National Institute of Polar Research; Tokyo Japan
| | - H. Miyaoka
- National Institute of Polar Research; Tokyo Japan
| | - K. Yumoto
- Space Environment Research Center; Kyushu University; Fukuoka Japan
| | - G. K. Parks
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - F. Honary
- Department of Physics; Lancaster University; Lancaster UK
| | - J. G. Trotignon
- Laboratoire de Physique et Chimie de l'Environnement et de l'Espace; Orléans France
| | - P. M. E. Décréau
- Laboratoire de Physique et Chimie de l'Environnement et de l'Espace; Orléans France
| | - B. W. Reinisch
- Center for Atmospheric Research; University of Massachusetts Lowell; Lowell Massachusetts USA
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23
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Mende SB, Frey HU, Angelopoulos V, Nishimura Y. Substorm triggering by poleward boundary intensification and related equatorward propagation. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010ja015733] [Citation(s) in RCA: 45] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- S. B. Mende
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - H. U. Frey
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - V. Angelopoulos
- Institute of Geophysics and Planetary Physics; University of California; Los Angeles California USA
| | - Y. Nishimura
- Department of Atmospheric and Oceanic Sciences; University of California; Los Angeles California USA
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24
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Zou S, Moldwin MB, Lyons LR, Nishimura Y, Hirahara M, Sakanoi T, Asamura K, Nicolls MJ, Miyashita Y, Mende SB, Heinselman CJ. Identification of substorm onset location and preonset sequence using Reimei, THEMIS GBO, PFISR, and Geotail. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010ja015520] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- S. Zou
- Department of Atmospheric, Oceanic and Space Sciences; University of Michigan; Ann Arbor Michigan USA
| | - M. B. Moldwin
- Department of Atmospheric, Oceanic and Space Sciences; University of Michigan; Ann Arbor Michigan USA
| | - L. R. Lyons
- Department of Atmospheric and Oceanic Sciences; University of California; Los Angeles California USA
| | - Y. Nishimura
- Department of Atmospheric and Oceanic Sciences; University of California; Los Angeles California USA
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - M. Hirahara
- Department of Earth and Planetary Science; University of Tokyo; Tokyo Japan
| | - T. Sakanoi
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - K. Asamura
- Institute of Space and Astronautical Science; Sagamihara Japan
| | - M. J. Nicolls
- Center for Geospace Studies; SRI International; Menlo Park California USA
| | - Y. Miyashita
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - S. B. Mende
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - C. J. Heinselman
- Center for Geospace Studies; SRI International; Menlo Park California USA
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25
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Morioka A, Miyoshi Y, Miyashita Y, Kasaba Y, Misawa H, Tsuchiya F, Kataoka R, Kadokura A, Mukai T, Yumoto K, Menietti DJ, Parks G, Liou K, Honary F, Donovan E. Two-step evolution of auroral acceleration at substorm onset. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010ja015361] [Citation(s) in RCA: 20] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- A. Morioka
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - Y. Miyoshi
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - Y. Miyashita
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - Y. Kasaba
- Geophysical Institute; Tohoku University; Sendai Japan
| | - H. Misawa
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - F. Tsuchiya
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - R. Kataoka
- Interactive Research Center; Tokyo Institute of Technology; Tokyo Japan
| | - A. Kadokura
- National Institute of Polar Research; Tokyo Japan
| | - T. Mukai
- Japan Aerospace Exploration Agency; Tokyo Japan
| | - K. Yumoto
- Space Environment Research Center; Kyushu University; Fukuoka Japan
| | - D. J. Menietti
- Department of Physics and Astronomy; University of Iowa; Iowa City Iowa USA
| | - G. Parks
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - K. Liou
- Johns Hopkins University Applied Physics Laboratory; Laurel Maryland USA
| | - F. Honary
- Department of Communication Systems; Lancaster University; Lancaster UK
| | - E. Donovan
- Department of Physics and Astronomy; University of Calgary; Calgary, Alberta Canada
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26
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Slavin JA, Anderson BJ, Baker DN, Benna M, Boardsen SA, Gloeckler G, Gold RE, Ho GC, Korth H, Krimigis SM, McNutt RL, Nittler LR, Raines JM, Sarantos M, Schriver D, Solomon SC, Starr RD, Trávnícek PM, Zurbuchen TH. MESSENGER observations of extreme loading and unloading of Mercury's magnetic tail. Science 2010; 329:665-8. [PMID: 20647422 DOI: 10.1126/science.1188067] [Citation(s) in RCA: 151] [Impact Index Per Article: 10.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
During MESSENGER's third flyby of Mercury, the magnetic field in the planet's magnetic tail increased by factors of 2 to 3.5 over intervals of 2 to 3 minutes. Magnetospheric substorms at Earth are powered by similar tail loading, but the amplitude is lower by a factor of approximately 10 and typical durations are approximately 1 hour. The extreme tail loading observed at Mercury implies that the relative intensity of substorms must be much larger than at Earth. The correspondence between the duration of tail field enhancements and the characteristic time for the Dungey cycle, which describes plasma circulation through Mercury's magnetosphere, suggests that such circulation determines the substorm time scale. A key aspect of tail unloading during terrestrial substorms is the acceleration of energetic charged particles, but no acceleration signatures were seen during the MESSENGER flyby.
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Affiliation(s)
- James A Slavin
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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27
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Kataoka R, Miyoshi Y, Morioka A. Hilbert-Huang Transform of geomagnetic pulsations at auroral expansion onset. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009ja014214] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ryuho Kataoka
- Interactive Research Center of Science; Tokyo Institute of Technology; Tokyo Japan
| | | | - Akira Morioka
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
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28
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Comparative study of a substorm event by satellite observation and model simulation. CHINESE SCIENCE BULLETIN-CHINESE 2009. [DOI: 10.1007/s11434-009-0282-4] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/20/2022]
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29
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Slavin JA, Acuña MH, Anderson BJ, Baker DN, Benna M, Boardsen SA, Gloeckler G, Gold RE, Ho GC, Korth H, Krimigis SM, McNutt RL, Raines JM, Sarantos M, Schriver D, Solomon SC, Trávnícek P, Zurbuchen TH. MESSENGER observations of magnetic reconnection in Mercury's magnetosphere. Science 2009; 324:606-10. [PMID: 19407194 DOI: 10.1126/science.1172011] [Citation(s) in RCA: 205] [Impact Index Per Article: 13.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Solar wind energy transfer to planetary magnetospheres and ionospheres is controlled by magnetic reconnection, a process that determines the degree of connectivity between the interplanetary magnetic field (IMF) and a planet's magnetic field. During MESSENGER's second flyby of Mercury, a steady southward IMF was observed and the magnetopause was threaded by a strong magnetic field, indicating a reconnection rate ~10 times that typical at Earth. Moreover, a large flux transfer event was observed in the magnetosheath, and a plasmoid and multiple traveling compression regions were observed in Mercury's magnetotail, all products of reconnection. These observations indicate that Mercury's magnetosphere is much more responsive to IMF direction and dominated by the effects of reconnection than that of Earth or the other magnetized planets.
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Affiliation(s)
- James A Slavin
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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30
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Miyashita Y, Machida S, Kamide Y, Nagata D, Liou K, Fujimoto M, Ieda A, Saito MH, Russell CT, Christon SP, Nosé M, Frey HU, Shinohara I, Mukai T, Saito Y, Hayakawa H. A state-of-the-art picture of substorm-associated evolution of the near-Earth magnetotail obtained from superposed epoch analysis. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008ja013225] [Citation(s) in RCA: 99] [Impact Index Per Article: 6.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Y. Miyashita
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
| | - S. Machida
- Department of Geophysics; Kyoto University; Kyoto Japan
| | - Y. Kamide
- Research Institute for Sustainable Humanosphere; Kyoto University; Kyoto Japan
| | - D. Nagata
- Department of Geophysics; Kyoto University; Kyoto Japan
| | - K. Liou
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - M. Fujimoto
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
| | - A. Ieda
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - M. H. Saito
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
| | - C. T. Russell
- Institute of Geophysics and Planetary Physics; University of California; Los Angeles California USA
| | | | - M. Nosé
- Data Analysis Center for Geomagnetism and Space Magnetism, Graduate School of Science; Kyoto University; Kyoto Japan
| | - H. U. Frey
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - I. Shinohara
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
| | - T. Mukai
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
| | - Y. Saito
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
| | - H. Hayakawa
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Kanagawa Japan
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31
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Affiliation(s)
- V. V. Anh
- School of Mathematical Sciences; Queensland University of Technology; Brisbane Queensland Australia
| | - J. M. Yong
- Department of Mathematics; University of Central Florida; Orlando Florida USA
| | - Z. G. Yu
- School of Mathematical Sciences; Queensland University of Technology; Brisbane Queensland Australia
- School of Mathematics and Computational Science; Xiangtan University; Hunan China
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Morioka A, Miyoshi Y, Tsuchiya F, Misawa H, Yumoto K, Parks GK, Anderson RR, Menietti JD, Donovan EF, Honary F, Spanswick E. AKR breakup and auroral particle acceleration at substorm onset. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008ja013322] [Citation(s) in RCA: 15] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- A. Morioka
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - Y. Miyoshi
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya Japan
| | - F. Tsuchiya
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - H. Misawa
- Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
| | - K. Yumoto
- Space Environment Research Center; Kyushu University; Fukuoka Japan
| | - G. K. Parks
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - R. R. Anderson
- Department of Physics and Astronomy; University of Iowa; Iowa City Iowa USA
| | - J. D. Menietti
- Department of Physics and Astronomy; University of Iowa; Iowa City Iowa USA
| | - E. F. Donovan
- Department of Physics and Astronomy; University of Calgary; Calgary, Alberta Canada
| | - F. Honary
- Department of Communication Systems; Lancaster University; Lancaster UK
| | - E. Spanswick
- Department of Physics and Astronomy; University of Calgary; Calgary, Alberta Canada
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Ieda A, Fairfield DH, Slavin JA, Liou K, Meng CI, Machida S, Miyashita Y, Mukai T, Saito Y, Nosé M, Shue JH, Parks GK, Fillingim MO. Longitudinal association between magnetotail reconnection and auroral breakup based on Geotail and Polar observations. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008ja013127] [Citation(s) in RCA: 24] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- A. Ieda
- Solar-Terrestrial Environment Laboratory; Nagoya University; Nagoya, Aichi Japan
| | - D. H. Fairfield
- Heliophysics Science Division; NASA Goddard Space Flight Center; Greenbelt Maryland USA
| | - J. A. Slavin
- Heliophysics Science Division; NASA Goddard Space Flight Center; Greenbelt Maryland USA
| | - K. Liou
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - C.-I. Meng
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - S. Machida
- Department of Geophysics; Kyoto University; Kyoto Japan
| | - Y. Miyashita
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Sagamihara, Kanagawa Japan
| | - T. Mukai
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Sagamihara, Kanagawa Japan
| | - Y. Saito
- Institute of Space and Astronautical Science; Japan Aerospace Exploration Agency; Sagamihara, Kanagawa Japan
| | - M. Nosé
- Data Analysis Center for Geomagnetism and Space Magnetism, Graduate School of Science; Kyoto University; Kyoto Japan
| | - J.-H. Shue
- Institute of Space Science; National Central University; Jhongli Taiwan
| | - G. K. Parks
- Space Sciences Laboratory; University of California; Berkeley California USA
| | - M. O. Fillingim
- Space Sciences Laboratory; University of California; Berkeley California USA
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Angelopoulos V, McFadden JP, Larson D, Carlson CW, Mende SB, Frey H, Phan T, Sibeck DG, Glassmeier KH, Auster U, Donovan E, Mann IR, Rae IJ, Russell CT, Runov A, Zhou XZ, Kepko L. Tail reconnection triggering substorm onset. Science 2008; 321:931-5. [PMID: 18653845 DOI: 10.1126/science.1160495] [Citation(s) in RCA: 476] [Impact Index Per Article: 29.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Magnetospheric substorms explosively release solar wind energy previously stored in Earth's magnetotail, encompassing the entire magnetosphere and producing spectacular auroral displays. It has been unclear whether a substorm is triggered by a disruption of the electrical current flowing across the near-Earth magnetotail, at approximately 10 R(E) (R(E): Earth radius, or 6374 kilometers), or by the process of magnetic reconnection typically seen farther out in the magnetotail, at approximately 20 to 30 R(E). We report on simultaneous measurements in the magnetotail at multiple distances, at the time of substorm onset. Reconnection was observed at 20 R(E), at least 1.5 minutes before auroral intensification, at least 2 minutes before substorm expansion, and about 3 minutes before near-Earth current disruption. These results demonstrate that substorms are likely initiated by tail reconnection.
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Affiliation(s)
- Vassilis Angelopoulos
- Institute of Geophysics and Planetary Physics/ESS, University of California at Los Angeles, Los Angeles, CA 90095, USA.
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Zhang L, Liu Z, Wang J, Ma Z, Pu Z, Shen C, Guo J. The distribution characteristics of the flows in the near-Earth region: TC-1 observational results. CHINESE SCIENCE BULLETIN-CHINESE 2007. [DOI: 10.1007/s11434-007-0433-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/22/2022]
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Zhang Y, Liu Z, Shen C, Duan S, He Z, Carr CM, Réme H. Double Star TC-1 observation of the earthward flowing plasmoids in the near magnetotail. CHINESE SCIENCE BULLETIN-CHINESE 2007. [DOI: 10.1007/s11434-007-0212-2] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/23/2022]
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Zhang H, Pu Z, Cao X, Fu S, Xiao C, Liu Z, Korth A, Frazen M, Zong Q, Reme H, Glassmeier KH, Friedel R, Reeves GD, Dunlop MW. Correlation between continuous lobe reconnection in the mid magnetotail and substorm expansion onset. CHINESE SCIENCE BULLETIN-CHINESE 2006. [DOI: 10.1007/s11434-006-2198-6] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/23/2022]
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Taylor MGGT, Reeves GD, Friedel RHW, Thomsen MF, Elphic RC, Davies JA, Dunlop MW, Laakso H, Lavraud B, Baker DN, Slavin JA, Perry CH, Escoubet CP, Masson A, Opgenoorth HJ, Vallat C, Daly PW, Fazakerley AN, Lucek EA. Cluster encounter with an energetic electron beam during a substorm. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006ja011666] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Pulkkinen A, Klimas A, Vassiliadis D, Uritsky V. Role of stochastic fluctuations in the magnetosphere-ionosphere system: A stochastic model for theAEindex variations. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006ja011661] [Citation(s) in RCA: 31] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Goldstein J. Coupled response of the inner magnetosphere and ionosphere on 17 April 2002. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004ja010712] [Citation(s) in RCA: 75] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Slavin JA. Cluster observations of traveling compression regions in the near-tail. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004ja010878] [Citation(s) in RCA: 66] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Shiokawa K, Yago K, Yumoto K, Baishev DG, Solovyev SI, Rich FJ, Mende SB. Ground and satellite observations of substorm onset arcs. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005ja011281] [Citation(s) in RCA: 11] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Daglis IA, Kozyra JU, Kamide Y, Vassiliadis D, Sharma AS, Liemohn MW, Gonzalez WD, Tsurutani BT, Lu G. Intense space storms: Critical issues and open disputes. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002ja009722] [Citation(s) in RCA: 77] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- I. A. Daglis
- Institute for Space Applications and Remote Sensing; National Observatory of Athens, Penteli; Athens Greece
| | - J. U. Kozyra
- Space Physics Research Laboratory; University of Michigan; Ann Arbor Michigan USA
| | - Y. Kamide
- Solar-Terrestrial Environment Laboratory; Nagoya University; Toyokawa Japan
| | - D. Vassiliadis
- USRA at NASA Goddard Space Flight Center; Greenbelt Maryland USA
| | - A. S. Sharma
- University of Maryland; College Park Maryland USA
| | - M. W. Liemohn
- Space Physics Research Laboratory; University of Michigan; Ann Arbor Michigan USA
| | - W. D. Gonzalez
- Instituto de Pesquisas Espaciais; Sao Jose dos Campos; Sao Paulo Brazil
| | | | - G. Lu
- High-Altitude Observatory; NCAR; Boulder Colorado USA
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Shao X. Phase transition-like behavior of magnetospheric substorms: Global MHD simulation results. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2001ja009237] [Citation(s) in RCA: 17] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cson Brandt P, Demajistre R, Roelof EC, Ohtani S, Mitchell DG, Mende S. IMAGE/high-energy energetic neutral atom: Global energetic neutral atom imaging of the plasma sheet and ring current during substorms. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2002ja009307] [Citation(s) in RCA: 35] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- P. Cson Brandt
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - R. Demajistre
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - E. C. Roelof
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - S. Ohtani
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - D. G. Mitchell
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - S. Mende
- Space Science Laboratory; Berkeley California USA
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